Chemical Evolution in Sersic 159-03 Observed with Xmm-Newton

Plaa, J. de; Werner, N; Bykov, A M; Kaastra, J S; Mendez, M; Vink, J; Bleeker, J; Bonamente, M; Peterson, J R

doi:10.2172/877208

Cited by 2 publications

(2 citation statements)

References 43 publications

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“…A comparison of the wdem model with the classical coolingflow model can be found in de Plaa et al (2005). We note that the wdem model contains less cool gas than the classical cooling-flow model, which is consistent with recent observations (Peterson et al 2001(Peterson et al , 2003.…”

Section: Spectral Modelssupporting

confidence: 87%

XMM-Newton Spectroscopy of the Cluster of Galaxies 2a 0335+096

Werner¹,

Plaa²,

Kaastra³

et al. 2006

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Abstract. We present here the results of a deep (130 ks) XMM-Newton observation of the cluster of galaxies 2A 0335+096. The deep exposure allows us to study in detail its temperature structure and its elemental abundances. We fit three different thermal models and find that the multi-temperature wdem model fits our data best. We find that the abundance structure of the cluster is consistent with a scenario where the relative number of Type Ia supernovae contributing to the enrichment of the intra-cluster medium is ∼ 25%, while the relative number of core collapse supernovae is ∼ 75%. Comparison of the observed abundances to the supernova yields does not allow us to put any constrains on the contribution of Pop III stars to the enrichment of the ICM. Radial abundance profiles show a strong central peak of both Type Ia and core collapse supernova products. Both the temperature and iron abundance maps show an asymmetry in the direction of the elongated morphology of the surface brightness. In particular the temperature map shows a sharp change over a brightness edge on the southern side of the core, which was identified as a cold front in the Chandra data. This suggests that the cluster is in the process of a merger with a subcluster. Moreover, we find that the blobs or filaments discovered in the core of the cluster by Chandra are, contrary to the previous results, colder than the ambient gas and they appear to be in pressure equilibrium with their environment.

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Section: Spectral Modelssupporting

confidence: 87%

XMM-Newton Spectroscopy of the Cluster of Galaxies 2a 0335+096

Werner¹,

Plaa²,

Kaastra³

et al. 2006

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“…X-ray observations of the galaxy clusters (see e.g. de Plaa et al, 2006;Böhringer and Werner, 2010;Mernier et al, 2017) provided clear evidences that the ICM does not have a primordial composition, but has been enriched with metals up to about 1.5 -2 times of the solar abundance.…”

Section: Hybrid Simulations Of Shocks In Hot Multicomponent Plasmasmentioning

confidence: 99%

Shocks and Non-thermal Particles in Clusters of Galaxies

et al. 2019

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Galaxy clusters grow by gas accretion, mostly from mergers of substructures, which release powerful shock waves into cosmic plasmas and convert a fraction of kinetic energy into thermal energy, amplification of magnetic fields and into the acceleration of energetic particles. The modeling of the radio signature of cosmic shocks, combined with the lack of detected γ-rays from cosmic ray (CR) protons, poses challenges to our understanding of how cosmic rays get accelerated and stored in the intracluster medium. Here we review the injection of CRs by cosmic shocks of different strengths, combining the detailed "microscopic" view of collisionless processes governing the creation of non-thermal distributions of electrons and protons in cluster shocks (based on analytic theory and particle-in-cell simulations), with the "macroscopic" view of the large-scale distribution of cosmic rays, suggested by modern cosmological simulations. Time dependent non-linear kinetic models of particle acceleration by multiple internal shocks with large scale compressible motions of plasma with soft CR spectra containing a noticable energy density in the superthermal protons of energies below a few GeV which is difficult to constrain by Fermi

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Chemical Evolution in Sersic 159-03 Observed with Xmm-Newton

Cited by 2 publications

References 43 publications

XMM-Newton Spectroscopy of the Cluster of Galaxies 2a 0335+096

XMM-Newton Spectroscopy of the Cluster of Galaxies 2a 0335+096

Shocks and Non-thermal Particles in Clusters of Galaxies

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